1912.01621.pdf

Draft version March 16, 2020

Typeset using L

twocolumn

style in AASTeX63

The ALPINE-ALMA [CII] Survey:

Multi-Wavelength Ancillary Data and Basic Physical Measurements

A. L. Faisst

D. Schaerer

2, 3

B. C. Lemaux

P. A. Oesch

Y. Fudamoto

P. Cassata

5, 6

M. B

ethermin

P. L. Capak

1, 8, 9

O. Le F

evre

J. D. Silverman

10, 11

L. Yan

M. Ginolfi,

A. M. Koekemoer

L. Morselli,

5, 6

R. Amor

ın

14, 15

S. Bardelli

M. Boquien

G. Brammer

A. Cimatti,

18, 19

M. Dessauges-Zavadsky

S. Fujimoto

8, 9

C. Gruppioni

N. P. Hathi

S. Hemmati

E. Ibar,

G. C. Jones

22, 23

Y. Khusanova,

7, 24

F. Loiacono,

18, 16

F. Pozzi

M. Talia

18, 16

L. A. M. Tasca,

D. A. Riechers

25, 24

G. Rodighiero

5, 6

M. Romano,

5, 6

N. Scoville

S. Toft

8, 9

L. Vallini

D. Vergani,

G. Zamorani

and E. Zucca

IPAC, M/C 314-6, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA

Observatoire de Gen`eve, Universit ́e de Gen`eve, 51 Ch. des Maillettes, 1290 Versoix, Switzerland

Institut de Recherche en Astrophysique et Plan ́etologie

−

IRAP, CNRS, Universit ́e de Toulouse, UPS-OMP, 14, avenue E. Belin,

F31400 Toulouse, France

Department of Physics, University of California, Davis, One Shields Ave., Davis, CA 95616, USA

Dipartimento di Fisica e Astronomia, Universit`a di Padova, vicolo dell’Osservatorio, 3 I-35122 Padova, Italy

INAF, Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy

Aix Marseille Universit ́e, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388, Marseille, France

The Cosmic Dawn Center, University of Copenhagen, Vibenshuset, Lyngbyvej 2, DK-2100 Copenhagen, Denmark

Niels Bohr Institute, University of Copenhagen, Lyngbyvej 2, DK-2100 Copenhagen, Denmark

Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa, Japan 277-8583 (Kavli IPMU,

WPI)

Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan

The Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA

Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

Instituto de Investigaci ́on Multidisciplinar en Ciencia y Tecnolog ́ıa, Universidad de La Serena, Ra ́ul Bitr ́an 1305, La Serena, Chile

Departamento de Astronom ́ıa, Universidad de La Serena, Av. Juan Cisternas 1200 Norte, La Serena, Chile

INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 93/3, I-40129, Bologna, Italy

Centro de Astronom ́ıa (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta, Chile

Universit`a di Bologna - Dipartimento di Fisica e Astronomia, Via Gobetti 93/2 - I-40129, Bologna, Italy

INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125, Firenze, Italy

Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA

Instituto de F ́ısica y Astronom ́ıa, Universidad de Valpara ́ıso, Avda. Gran Breta ̃na 1111, Valpara ́ıso, Chile

Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge CB3 0HE, UK

Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

Max-Planck-Institut f ̈ur Astronomie, K ̈onigstuhl 17, D-69117 Heidelberg, Germany

Department of Astronomy, Cornell University, Space Sciences Building, Ithaca, NY 14853, USA

California Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USA

Leiden Observatory, Leiden University, PO Box 9500, 2300 RA Leiden, The Netherlands

Submitted to ApJS

ABSTRACT

We present the ancillary data and basic physical measurements for the galaxies in the

ALMA Large

Program to Investigate C

at Early Times (ALPINE)

survey

−

the first large multi-wavelength survey

which aims at characterizing the gas and dust properties of 118 main-sequence galaxies at redshifts

< z <

9 via the measurement of [C

] emission at 158

m (64% at

) and the surrounding

Corresponding author: Andreas L. Faisst

afaisst@ipac.caltech.edu

arXiv:1912.01621v2 [astro-ph.GA] 13 Mar 2020

Faisst et al.

far-infrared (FIR) continuum in conjunction with a wealth of optical and near-infrared data. We

outline in detail the spectroscopic data and selection of the galaxies as well as the ground- and space-

based imaging products. In addition, we provide several basic measurements including stellar masses,

star formation rates (SFR), rest-frame ultra-violet (UV) luminosities, UV continuum slopes (

), and

absorption line redshifts, as well as H

emission derived from Spitzer colors. We find that the

ALPINE

sample is representative of the 4

< z <

6 galaxy population selected by photometric methods and only

slightly biased towards bluer colors (∆

∼

2). Using [C

] as tracer of the systemic redshift (confirmed

for one galaxy at

= 4

5 out of 118 for which we obtained optical [O

]

3727

A emission), we confirm

red shifted Ly

emission and blue shifted absorption lines similar to findings at lower redshifts. By

stacking the rest-frame UV spectra in the [C

] rest-frame we find that the absorption lines in galaxies

with high specific SFR are more blue shifted, which could be indicative of stronger winds and outflows.

Keywords:

galaxies: evolution — galaxies: fundamental parameters — galaxies: ISM — galaxies: star

formation — galaxies: photometry

INTRODUCTION

1.1.

The Early Growth Phase in Galaxy Evolution

Galaxy evolution undergoes several important phases

such as the ionization of neutral Hydrogen at redshifts

z >

6 (also known as the Epoch of Reionizaton) as well

as a time of highest cosmic star-formation rate (SFR)

density at

∼

−

3. The transition phase at

= 4

−

(a time roughly 0

9 to 1

5 billion years after the Big

Bang), often referred to as the

early growth phase

, is

currently in focus of many studies. This time is of great

interest for understanding galaxy evolution as it con-

nects primordial galaxy formation during the epoch of

reionization with mature galaxy growth at and after the

peak of cosmic SFR density. During a time of only

600 Myrs, the cosmic stellar mass density in the uni-

verse increased by one order of magnitude (Caputi et al.

2011; Davidzon et al. 2017), galaxies underwent a critical

morphological transformation to build up their disk and

bulge structures (Gnedin et al. 1999; Bournaud et al.

2007; Agertz et al. 2009), and their interstellar medium

(ISM) became enriched with metal from sub-solar to so-

lar amounts (Ando et al. 2007; Faisst et al. 2016a), while

at the same time the dust attenuation of the UV light

significantly increased (Finkelstein et al. 2012; Bouwens

et al. 2015; Fudamoto et al. 2017; Popping et al. 2017;

Cullen et al. 2018; Ma et al. 2019; Yamanaka & Yamada

2019). Furthermore, the most massive of these galaxies

may become the first quiescent galaxies already at

z >

(Glazebrook et al. 2017; Valentino et al. 2019; Tanaka

et al. 2019; Stockmann et al. 2020; Faisst et al. 2019).

All this put together, makes the early growth phase an

important puzzle piece to be studied in order to decipher

how galaxies formed and evolved to become the galaxies

(either star forming or quiescent) that we observe in the

local universe.

It is evident from studies at lower redshift that multi-

wavelength observations are crucial for us to be able to

form a coherent picture of galaxy evolution. To capture

several important properties of galaxies, a

panchromatic

survey must comprise several spectroscopic and imaging

datasets that cover a large fraction of the wavelength

range of a galaxy’s light emission, including

(i)

the rest-

frame ultra-violet (UV) containing Ly

emission, as well

as several absorption lines to study stellar winds and

metallicity (Heckman et al. 1997; Maraston et al. 2009;

Steidel et al. 2010; Faisst et al. 2016a),

(ii)

the rest-

frame optical containing tracers of age (Balmer break)

as well as important emission lines (e.g., H

) to quantify

the star-formation and gas metal properties (Kennicutt

1998; Kewley & Ellison 2008), and

(iii)

the far-infrared

(FIR) continuum and several FIR emission lines (e.g,.

]

158

m or [N

]

205

m) that provide insights into

the gas and dust properties of galaxies (De Looze et al.

2014; Pavesi et al. 2019).

Fortunately, the early growth phase at redshifts

= 4

−

6 is at the same time the highest red-

shift epoch at which, using current technologies, such a

panchromatic study can be carried out. The rest-frame

UV part of the energy distribution at these redshifts has

been probed in the past thanks to several large spec-

troscopic (Le F`evre et al. 2015; Hasinger et al. 2018)

and imaging (Capak et al. 2007; McCracken et al. 2012;

Aihara et al. 2019) surveys from the ground as well as

imaging surveys with the Hubble Space Telescope (HST,

Grogin et al. 2011; Koekemoer et al. 2011; Scoville et al.

2007a). In addition, H

has been accessed successfully

through observations with the Spitzer Space Telescope

(Stark et al. 2013; de Barros et al. 2014; Smit et al.

2014; Rasappu et al. 2016; Smit et al. 2016; Faisst et al.

2016a, 2019; Lam et al. 2019). However, the FIR of

z >

4 galaxies has only been probed sparsely in the past

in less than a dozen galaxies using the

Atacama Large

The ALPINE-ALMA [CII] Survey: Ancillary Data

* Typical z = 5 galaxy

α

optical

emission

lines

UV continuum

and

Absorption

lines

Magnitude

Observed wavelength [

100

1000

α

[CII]

gas, dust,

dust obscured

star formation

hot gas and

star formation

stars, dust,

metallicity,

stellar winds

FIR continuum

and lines

Sections in this paper are indicated

Spectroscopy

(Keck/DEIMOS, VUDS, GOODS-S/VLT)

§2

Imaging

(ground & HST; various programs)

§3

Spitzer imaging -

§3

α

from Spitzer colors -

§4

Layout of Current Data Products for

ALPINE

Galaxies

SED fitting -

§4

(Stellar masses, SFR)

ALMA

Data reduction:

Béthermin et al. (2019)

Figure 1.

ALPINE

builds the corner stone of a panchromatic survey at

= 4

−

6. The diagram shows the multi-wavelength

data products that are currently available for all the

ALPINE

galaxies. The currently covered parts of the spectrum are

indicated in red. The numbers link to sections in this paper where the data products and their analysis are explained in detail.

The spectrum sketch is based on a typical

= 5 galaxy (adapted from Harikane et al. 2018).

(Sub-) Millimeter Array

(ALMA, Riechers et al. 2014;

Capak et al. 2015; Watson et al. 2015; Willott et al.

2015; Strandet et al. 2017; Carniani et al. 2018; Zavala

et al. 2018b,a; Casey et al. 2019; Jin et al. 2019) as

well as some as part of Herschel surveys in lensed and

unlensed fields (e.g., Egami et al. 2010; Combes et al.

2012; Casey et al. 2012, 2014). Commonly targeted by

observations with ALMA is singly ionized Carbon (C

)

at 158

m, which is an important coolant for the gas in

galaxies and is therefore broadly related to star forma-

tion activity and gas masses (Stacey et al. 1991; Carilli

& Walter 2013; De Looze et al. 2014). The [C

] emis-

sion line is one of the strongest in the FIR and is in

addition conveniently located in the ALMA Band 7 at

redshifts

= 4

−

6 at one of the highest atmospheric

transmissions compared to other FIR lines (see, e.g.,

Faisst et al. 2017). The origin of [C

] emission is still de-

bated. In addition to photo-dissociation regions (PDRs)

and the cold neutral medium, a significant fraction can

also origin from ionized gas regions or CO-dark molecu-

lar clouds (Pineda et al. 2013; Vallini et al. 2015; Pavesi

et al. 2016). Also, the increasing temperature of the Cos-

mic Microwave Background (CMB) has an effect on the

relation between [C

] and star formation (Ferrara et al.

2019). Both potentially complicates the interpretation

of [C

] as SFR indicator at high redshifts. Similar to

, [C

] traces the gas kinematics in a galaxy and is

therefore an important component to quantify rotation-

and dispersion-dominated systems as well as outflows

(Jones et al. 2017; Pavesi et al. 2018; Kohandel et al.

2019; Ginolfi et al. 2019).

The FIR landscape has dramatically changed with

the completion of the

ALMA Large Program to Inves-

tigate C

at Early Times

(

ALPINE

, #2017.1.00428.L).

ALPINE

is laying the ground work for the exploration of

gas and dust properties in 118

main-sequence

star form-

ing galaxies in the early growth phase at 4

< z <

and herewith started the first panchromatic survey of

its kind at these redshifts.

1.2.

ALPINE in a Nutshell

Faisst et al.

In the following, we summarize the scope of the

ALPINE

survey, we refer to Le F`evre et al. (2019) for a

broader overview of the program.

ALPINE

is a 69 hour

large ALMA program started in Cycle 5 in May 2018

and completed during Cycle 6 in February 2019. In to-

tal, 118 galaxies have been observed in Band 7 (cover-

ing [C

] emission at 158

m and its nearby continuum)

at a spatial resolution of

′′

and with integration

times

∼

30 minutes on-source depending on their pre-

dicted [C

] flux. The galaxies origin from two fields,

namely the

Cosmic Evolution Survey

field (COSMOS,

105 galaxies, Scoville et al. 2007b) and the

Extended

Chandra Deep Field South

(ECDFS, 13 galaxies, Giac-

coni et al. 2002). Due to gaps in the transition through

the atmosphere, the galaxies are split in two different

redshift ranges spanning 4

< z <

65 and 5

< z <

90 with medians of

〈

〉

= 4

5 and 5

5 and galaxy num-

bers of 67 and 51, respectively. All galaxies are spectro-

scopically confirmed by either Ly

emission or rest-UV

absorption lines and are selected to be brighter than an

absolute UV magnitude of

1500

−

2. This limit is

roughly equivalent to a SFR cut at 10 M

−

and cor-

responds roughly to a limiting luminosity in [C

] emis-

sion of

[CII]

= 1

−

(assuming the relation

derived by De Looze et al. 2014). Assuming a 3

de-

tection limit, the [C

] detection rate is 64% and con-

tinuum emission is detected in 19% of the galaxies (see

Figure 2).

The main science goals enabled by

ALPINE

are di-

verse and cover many crucial research topics at high

redshifts:

−

connecting [C

] to star-formation at high red-

shifts,

−

coherent study of the total SFR density at

z >

including the contribution of dust-obscured star

formation,

−

study of gas dynamics and merger statistics from

] kinematics and quantification of UV-faint

companion galaxies,

−

study of gas fractions and dust properties at

z >

−

the first characterization of ISM properties using

FIR

and [C

]/FIR continuum diagnostics

for a large sample at

z >

−

quantifying outflows and feedback processes in

z >

4 galaxies from [C

] line profiles.

Note that

ALPINE

provides at the same time the

equivalent of a blind-survey of approximately 25 square-

arcminutes. This enables us to estimate the obscured

fraction of star-formation (mostly below

= 4) by find-

ing UV-faint galaxies with FIR continuum or [C

] emis-

sion. The serendipitous continuum sources and [C

] de-

tections are discussed in detail in Bethermin et al. (2020)

signal-to-noise ratio

Number

3.5

SNR for ALMA-detected (

> 3.5

) sources

[CII] line emission

FIR continuum emission

Figure 2.

Signal-to-Noise (SNR) of the ALMA-detected

sources in the

ALPINE

sample. The different histograms

show the numbers for [C

] and continuum detections above

. For more information, see Le F`evre et al. (2019) and

Bethermin et al. (2020).

and Loiacono et al. (in prep.). A more detailed descrip-

tion of these science goals can be found in our survey

overview paper (Le F`evre et al. 2019).

ALPINE

is based on a rich set of ancillary data, which

makes it the first panchromatic survey at these high red-

shifts including imaging and spectroscopic observations

at FIR wavelengths (see Figure 1). The backbone for a

successful selection of galaxies are rest-frame UV spec-

troscopic observations from the Keck telescope in Hawaii

as well as the European

Very Large Telescope

(VLT) in

Chile. These are complemented by ground-based imag-

ing observations from rest-frame UV to optical, HST

observations in the rest-frame UV, and Spitzer coverage

above the Balmer break at rest-frame 4000

A. The latter

is crucial for the robust measurement of stellar masses

at these redshifts (e.g., Faisst et al. 2016b).

For a survey overview of

ALPINE

see Le F`evre et al.

(2019) and for details on the data analysis see Bethermin

et al. (2020). In this paper, we present these valuable

ancillary data products and detail several basic mea-

surements for the

ALPINE

galaxies. The outline of the

paper is sketched in Figure 1. Specifically, in Section 2,

we present the spectroscopic data and detail the spectro-

scopic selection of the

ALPINE

galaxies. In the same

section, we also present stacked spectra and touch on

velocity offsets between Ly

, [C

], and absorption line

redshifts. Section 3 is devoted to the photometric data

products, which include ground- and space-based pho-

tometry. In Section 4.1, we detail the derivation of sev-

The ALPINE-ALMA [CII] Survey: Ancillary Data

eral galaxy properties from the observed photometry.

These include stellar masses, SFRs, UV luminosities,

UV continuum slopes, as well as H

emission derived

from Spitzer colors. We conclude and summarize in Sec-

tion 5. All presented data products are available in the

online printed version of this paper

. The different cata-

logs and their columns are described in detail in the Ap-

pendix A. HST cutouts and rest-frame UV spectra for

each of the

ALPINE

galaxies are shown in Appendix B.

Throughout the paper we assume the ΛCDM cos-

mology with

= 70 km s

−

Mpc

−

, Ω

= 0

70, and

Ω

= 0

30. All magnitudes are given in the AB system

(Oke 1974) and stellar masses and SFRs are normalized

to a Chabrier (2003) initial mass function (IMF).

SPECTROSCOPIC DATA AND SELECTION

2.1.

Spectroscopic selection of ALPINE galaxies

The

ALPINE

survey is only possible due to a spectro-

scopic pre-selection of galaxies from large spectroscopic

surveys on COSMOS and ECDFS. This is because the

ALMA frequency bands are narrow (

∼

1000 km s

−

and in order to observe [C

] emission the redshift has

to be known within a precision of

∼

1000 km

s. The

galaxy selection is refined to optimize the efficiency of

the ALMA observations by creating groups of galax-

ies in spectral dimensions. Our sample also includes

7 galaxies that were previously observed with ALMA

by Riechers et al. (2014) and Capak et al. (2015).

These are

HZ1

HZ2

HZ3

HZ4

HZ5

HZ6

LBG-1

and

HZ8

, which correspond to the

ALPINE

galax-

ies

536534

417567

683613

494057

845652

848185

, and

873321

, respectively.

Furthermore, four galaxies from the VUDS survey

(

5101288969

5100822662

, and

510786441

COSMOS and

530029038

in ECDFS) are observed

twice (resulting in a total number of 122 observations).

The duplicate observations are used for quality assess-

ment. Bethermin et al. (2020) describes the combination

of these observations.

The rest-frame UV spectroscopic data from which

the

ALPINE

sample is selected combine various large

surveys on the COSMOS and ECDFS fields. Out of

the 105

ALPINE

galaxies on the COSMOS field, 84

are obtained by the large DEIMOS spectroscopic sur-

vey (Capak et al. 2004; Mallery et al. 2012; Hasinger

et al. 2018) at the Keck telescope in Hawaii.

The

remaining spectra on the COSMOS field are ob-

tained from the VIMOS Ultra Deep Survey (VUDS,

Le F`evre et al. 2015; Tasca et al. 2017) at the VLT

http://www.astro.caltech.edu/

∼

afaisst/

Table 1.

Spectroscopy and selection of

ALPINE

galaxies

Survey

Selection

Number

Ref.

COSMOS field (105 galaxies)

Keck/DEIMOS

†

narrow-band (

∼

narrow-band (

∼

LBG (color)

pure photo-

m excess

X-ray (Chandra)

with Ly

emission

weak Ly

emission or absorption

VUDS

photo-

+ LBG

[narrow-band (

∼

‡

[narrow-band (

∼

‡

[LBG (color)

‡

m excess

‡

with Ly

emission

weak Ly

emission or absorption

ECDFS field (13 galaxies)

VLT GOODS-S

primarily LBG (color)

total with Ly

emission

total without Ly

emission

HST/GRAPES

Grism (no

a priori

selection)

with Ly

emission

weak Ly

emission or absorption

†

For a detailed description of the selection criteria, we refer to Mallery

et al. (2012) and Hasinger et al. (2018).

‡

Six of these galaxies are also observed as part of the Keck/DEIMOS

survey (ref.

1).

The corresponding number per selection from the

Keck/DEIMOS program is given in square-brackets for those six galaxies.

emitters selected with

NB711

emitters selected with

NB814

Color-selected galaxies in

, and

using the criteria

from Ouchi et al. (2004); Capak et al. (2004, 2011); Iwata et al. (2003);

Hildebrandt et al. (2009).

Galaxies with a photometric redshift

z >

4 with a probability of

50%

based on the Ilbert et al. (2010) photo-z catalog.

References: (1) Capak et al. (2004); Mallery et al. (2012); Hasinger et al.

(2018), (2) Le F`evre et al. (2015), (3) Vanzella et al. (2007, 2008); Balestra

et al. (2010), (4) Malhotra et al. (2005); Rhoads et al. (2009)

in Chile. In total 6 of the VUDS spectra are inde-

pendently also observed as part of the Keck/DEIMOS

survey (

5100559223

5100822662

5101218326

5101244930

5101288969

510786441

The

redshifts are consistent within 280 km s

−

and we do

not find any systematic offsets between the two obser-

vations (see also Section 2.4.1). Out of the 13 galax-

ies in the ECDFS field, 11 are obtained from spec-

troscopic observations with VIMOS (9) and FORS2

Faisst et al.

4.40

4.45

4.50

4.55

4.60

Spectroscopic Redshift

Number (stacked)

z ~ 4.5 sample

5.1

5.2

5.3

5.4

5.5

5.6

5.7

5.8

5.9

Spectroscopic Redshift

z ~ 5.5 sample

GRAPES (HST grism, ECDFS)

VLT VIMOS and FORS2 (ECDFS)

X-ray (Chandra)

LBG (color)

Narrow-band (low-z)

Narrow-band (high-z)

4.5

excess

photometric redshift

VUDS (photo-z + LBG)

Figure 3.

Redshift distribution of

ALPINE

galaxies. Each bar shows the stacked number of different selections per bin (see

Table 1 and description in text). The bins with galaxies from the ECDFS field are hatched. The left and right panels show

galaxies in the two different redshift bins.

z-band magnitude

K-band magnitude

GRAPES (HST grism, ECDFS)

VLT VIMOS and FORS2 (ECDFS)

X-ray (Chandra)

LBG (color)

Narrow-band (low-z)

Narrow-band (high-z)

4.5

excess

photometric redshift

VUDS (photo-z + LBG)

Parent (4 < z < 6)

9.5

10.0

10.5

11.0

11.5

12.0

log(

)

at rest-frame

1500 Å

9.5

10.0

10.5

11.0

11.5

12.0

log(

)

at rest-frame

4000 Å

GRAPES (HST grism, ECDFS)

VLT VIMOS and FORS2 (ECDFS)

X-ray (Chandra)

LBG (color)

Narrow-band (low-z)

Narrow-band (high-z)

4.5

excess

photometric redshift

VUDS (photo-z + LBG)

Figure 4.

Comparison of observed (i.e., not corrected for dust)

-band and

-band magnitudes (left) and luminosities (right)

for different selections listed in Table 1. The measurements on the parent sample in COSMOS at 4

< z <

6 is shown in light

gray. The color-coding is the same as in Figure 3. The arrows show 1

upper limits. The gray area denotes the

∗

, the knee

of the UV luminosity function, which corresponds to

−

15 (or log(

νL

)

∼

77) at

= 5 (Bouwens et al. 2015).

The derivation of the photometry is described in detail in Section 3.

) at the VLT (Vanzella et al. 2007, 2008; Balestra

et al. 2010), and 2 come from the HST grism survey

GRAPES

(Malhotra et al. 2005; Rhoads et al. 2009).

The spectral resolution of the different dataset varies

between

∼

100 (ECDFS/

GRAPES

grism),

∼

180 (ECDFS/VIMOS),

∼

230 (COSMOS/VUDS),

∼

660 (ECDFS/FORS2), and

∼

2500 (COS-

MOS/DEIMOS).

Biases towards dust-poor star-forming galaxies with

strong rest-frame UV emission lines (such as Ly

) can

One of these galaxies,

530029038

, has also been observed by

the VUDS survey.

be common in purely spectroscopically selected samples.

To minimized such biases as much as possible, the spec-

troscopically observed galaxies have been pre-selected

through a variety of different selection methods. The

largest fraction of galaxies in

ALPINE

is drawn from

the Keck/DEIMOS and VUDS surveys on the COS-

MOS field. Both surveys include galaxies preselected

in various ways, resulting in the most representative

and inclusive spectroscopic high-redshift galaxy sam-

ple. Specifically, the VUDS survey combines predom-

inantly a photometric redshift selection with a color-

selected Lyman Break Galaxy (LBG) selection (Le F`evre

et al. 2015), known as the Lyman-break drop-out tech-